where F\(_{\nu }\)  is the measured flux (normally at 1.3 mm), T\(_{\rm D}\)  is the dust temperature, \(k\)  is the Boltzmann constant, and \(\kappa _{\nu }\)  is the opacity. Total disk masses are determined from the previous expression for \(\sim \)  1/3 of the stars in the sample (those for which previous F\(_{\nu }\)  measurements are available). We adopted \(\kappa _{\rm 1.3mm}\)  = 0.02 cm\(^{-2}\) gr\(^{-1}\)  , which already includes a gas-to-dust ratio = 100, and a wavelength dependence \(\kappa _{\rm mm}\)  \(\propto \)  \(\lambda ^{-\beta }\)  [1]}i.e., opacities at different wavelengths are given by \(\kappa _{\lambda } = \kappa _{\rm 1.3mm}/(\lambda /1.3)^{-\beta }\), where 0 \(<\)  \(\beta \)  \(\le \)  2 is the dust opacity index associated with the typical dust grain size probed at (sub-) millimeter wavelengths (1.5-2 for the interstellar medium and smaller for larger grains). The values for T\(_{\rm D}\)  and \(\beta \)  are inferred from the best graybody model that fits the observed millimeter photometry using a \({\chi }^2\)  criterion [2]}, [3]}, [4]}. For the HAeBes with one single measurement of the millimeter flux, \(\beta \)  was fixed to 1 and T\(_{\rm D}\)  to the value in Table II of [5]} associated with the corresponding spectral type. The values of \(\beta \) , T\(_{\rm D}\)  and M\(_{\rm disk}\)  are listed in Cols 2, 3, and 4 of Table REF  whenever these estimates have been possible, and Cols 5 and 6 show the number of photometric points and the corresponding references that we used. The errors in M\(_{\rm disk}\)  were determined by propagation, considering only the uncertainties in the (sub-) millimeter fluxes. For the few flux values without associated error bars in the literature, typical \(\sim \)  10\(\%\)  uncertainties were assigned.
